Extragalactic X‐ray surveys: AGN physics and evolution

We review the most important findings on AGN physics and cosmological evolution as obtained by extragalactic X‐ray surveys and associated multiwavelength observations. We briefly discuss the perspectives for future enterprises and in particular the scientific case for an extremely deep (2–3 Ms) XMM survey. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Atmospheric Reactive Nitrogen Cycle and Stable Nitrogen Isotope Processes: Progresses and Perspectives

Oxidized reactive nitrogen in the atmosphere mainly consists of nitrogen oxides (NO _X =NO+NO₂, NO₃) and nitric acid. The atmospheric cycling of NO _X influences the formation of ozone and hydroxyl radicals that are important for atmospheric oxidation capacity. Nitric acid, the final product of NO _X oxidation, not only is an important component of particulate pollutants, but also has a direct impact on the ecosystem through dry and wet deposition. The stable nitrogen isotope (δ¹⁵N) shows the potential to study reactive nitrogen cycle, and to trace the emission, transport and deposition of reactive nitrogen from local to global scales. Here, we reviewed previous studies using δ¹⁵N to investigate NO _X emission and atmospheric reactive nitrogen cycle, and discuss the uncertainties of δ¹⁵N signatures of different NO _X sources from two aspects: NO _X generation mechanism and NO _X collection methods. We also discussed the nitrogen isotope fractionation and the consequences during the conversions of NO _y molecules. We ended up with discussions on the possibility of using δ¹⁵N to trace NO _X emissions. Although there are still large uncertainties in quantifying and tracing NO _X emissions using nitrogen stable isotopes, such isotope tool is efficient enough to trace reactive nitrogen cycles in the atmosphere. On the basis of this, we proposed that we can combine atmospheric chemistry transmission models with isotope tracers to improve our understanding of regional and global atmospheric reactive nitrogen cycle regarding the fluxes of different emission sources, their atmospheric transformation, etc.     

A ‘superoutburst’ in XTEJ1118+480

I propose that the properties of the two outbursts observed in the X‐ray transient XTEJ1118+480 in 2000 are akin to superoutbursts of SU UMa stars. In these systems a ‘normal’ outburst immediately precedes a 5–10 times longer (‘super’) outburst. The optical light curve of the outbursts of XTEJ1118+480 is remarkably similar to that seen in some SU UMa stars, such as UVPer and TLeo, where the precursor outburst is distinct from the superoutburst, but the time scales are a factor of ∼15 different. The first outburst of XTEJ1118+480 was relatively short (∼1 month) while the second outburst was ∼5 times longer. During the second outburst superhumps were seen, a feature characteristic for superoutbursts. The gap of about a month between the two outbursts is longer in X‐rays with respect to the optical, a feature not previously recognized for X‐ray transients. Also in SU UMa stars the precursor outburst becomes more distinct at shorter wavelengths. Finally, I show that the time of appearance of the superhumps in XTEJ1118+480 is consistent with the expected superhump growth time, if the superhump mechanism was triggered during the first outburst. I conclude that the similarity in outburst behaviour in the two types of systems provides further support that a common mechanism is at work to start the long (‘super’) outbursts.     

ROSAT HRI observations of P Cyg and surrounding area

We present a detailed analysis of deep ROSAT HRI observations of the luminous blue variable P Cyg and its surrounding radio nebula. The HRI image provides a point source at the position of P Cyg. However, we show that this emission can be attributed to the ultraviolet leak of the ROSAT HRI. The X‐ray flux upper limit derived from the HRI data of this star is discussed in the context of X‐ray emission from hot stars. Furthermore, we present a search for diffuse X‐ray emission possibly associated with the radio nebula surrounding P Cyg. We compare our results to model predictions and X‐ray fluxes observed for shells around other hot stars. Additionally, we detect 10 X‐ray sources in the field of view. All but one of these X‐ray emitters have stellar counter parts in the Palomar Sky Survey. We suggest that they are active late‐type stars possibly belonging to Cyg OB1.     

Variability of the Fe K line relativistic component in a sample of Seyfert 1 galaxies

We present the analysis of X‐ray spectral variability made on a sample of 7 Seyfert 1 bright galaxies, using XMM‐Newton data. From the “XMM‐Newton Science Archive” we selected those bright Seyfert 1 showing one or more prominent flares in their 2–10 keV light curves. For each of them we extracted spectra in 3 different time intervals: before, during and after the flare. We fitted them with a simple power law and then shifted a narrow emission and absorption line template across the 2.5–10 keV data, in order to investigate the presence of line‐like features with a confidence level greater than 99%. Some highly significant features were detected in 3 out of 7 sources studied. In particular, the 3 sources, namely PG 1211+143, NGC 4051 and NGC 3783, showed the presence of a variable emission feature in the 4.5–5.8 keV band, characterized by an increase of its intensity after the flare peak. Because of the observed variability pattern, this feature seems to be ascribable to a reverbered redshifted relativistic component of the Fe K line. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

QPO as the Rosetta Stone for understanding black hole accretion

Quasi‐periodic oscillations (QPO) seen in the X‐ray fluxes of individual neutron stars and black hole sources are one of most intriguing phenomena in today's astrophysics. The QPO nature is visibly determined by super‐strong Einstein's gravity. I argue here that it also profoundly depends on the MRI turbulence in accretion flows. Understanding the QPO physics may therefore guide accretion theory out of its present state of confusion. Readers will find here an up‐to‐date, comprehensible account of what is known, and what is not, about the QPO physics. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

我国各地膨润土的矿物学性质

运用X射线衍射分析技术对我国不同产地膨润土的矿物学性质进行考察；利用K值法测蒙脱石含量。实验表明，各地膨润土具有蒙脱石的含量较高且均为二八面体的矿物学特点；可能由于所处的矿层或局部地球化学环境不同，使得相同矿床的不同颜色膨润土矿物的蒙脱石含量有所差异。     

南极菲尔德斯半岛六种藻类和地衣植物的X荧光分析

为了研究南极的植物与环境间的关系 ,探讨植物在南极环境监测中的作用 ,在无标样条件下 ,利用微束 X荧光分析法对南极菲尔德斯半岛的 6种藻类和地衣植物进行了元素分析。其中藻类植物有孔石莼 (Ulva pertusa)、海膜 (H alymenia sp.)和大型鞘丝藻 (Lyngbya major) ,地衣植物有筛石蕊 (Cladonia borealis)、喇叭石蕊 (C.fimbriata)和松萝 (Usnea sp.)。研究结果发现 ,不同的藻类植物对各种元素的吸收能力不同 ,在 XRF(X射线荧光 )谱中 ,孔石莼比海膜含有更多的元素 ,象 As、Br和 Rb,Cu和 Zn的含量也较高。在大型鞘丝藻中 ,K比 Ca少 ,Zn的含量较高。在 3种地衣植物中 ,其 XRF谱中的元素种类组成非常相似 ,只是 Mn、Fe、Cu和 Zn等元素的相对含量有些差异     

利用高铁钾长石粉合成13X沸石分子筛的实验研究

对江苏丰县的富钾页岩进行预处理，得到钾长石含量达76．4％的钾长石粉，其Fe2O3含量高达7．52％。以此钾长石粉为原料经过焙烧处理、水热合成实验，在铁含量较高情况下成功合成了13X沸石分子筛，并采用正交实验法确定了优化工艺参数。对实验产物的主要性能测试表明，合成的富铁沸石产品与13X沸石分子筛工业产品相似，吸附量达到国家化学工业产品标准，可用于对含重金属离子废水的吸附处理。